已知a+b-2*根号a-1-4根号b-2=3根号c-3-1/2c-5求a+b+c的值_百度知道
已知a+b-2*根号a-1-4根号b-2=3根号c-3-1/2c-5求a+b+c的值
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a-1=1;+[√(b-2)-2]&#178,c-3=9
∴a=2;=0,√(c-3)-3=0;+&#189,√(c-3)=3,√(b-2)=2;[(c-3)-6√(c-3)+9]=0;c）-5,
同时平方得,√(b-2)-2=0,b=6,∴√(a-1)=1, ∴[√(a-1)-1]&#178， ∴a-1-2√(a-1)+1+b-2-4√(b-2)+4+&#189：∵a+b-2√(a-1)-4√(b-2)=3√(c-3)-（&#189，∴√(a-1)-1=0,b-2=4解;[√(c-3)-3]&#178
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2[根号(c-3)-3]^2=0,b=5配方得,a=2：[根号(a-1)-1]^2+[根号(b-1)-2]^2+1&#47,c=12a+b+c=19
配方得：[根号(a-1)-1]^2+[根号(b-1)-2]^2+1/2[根号(c-3)-3]^2=0,a=2,b=5,c=12a+b+c=19.
12（a=2,b=4,c=6）
你这根号管多少范围不讲清楚，只是根号后的字母么？
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出门在外也不愁Extinction dynamics of a discrete population in an oasis.
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):012722. Epub
2015 Jul 29.Extinction dynamics of a discrete population in an oasis.1, 2, 3, 4.1Laboratoire de Mécanique de Lille, CNRS/UMR 8107, Université Lille 1, 59650 Villeneuve d'Ascq, France.2Istituto dei Sistemi Complessi, CNR, Via dei Taurini 19, 00185, Rome, Italy.3Istituto per le Applicazioni del Calcolo, CNR, Via dei Taurini 19, 00185, Rome, Italy.4Dipartimento di Fisica, Università "La Sapienza," Piazzale Aldo Moro 2, I-00185 Roma, Italy and Istituto dei Sistemi Complessi, CNR, Via dei Taurini 19, 00185, Rome, Italy.AbstractUnderstanding the conditions ensuring the persistence of a population is an issue of primary importance in population biology. The first theoretical approach to the problem dates back to the 1950s with the Kierstead, Slobodkin, and Skellam (KiSS) model, namely a continuous reaction-diffusion equation for a population growing on a patch of finite size L surrounded by a deadly environment with infinite mortality, i.e., an oasis in a desert. The main outcome of the model is that only patches above a critical size allow for population persistence. Here we introduce an individual-based analog of the KiSS model to investigate the effects of discreteness and demographic stochasticity. In particular, we study the average time to extinction both above and below the critical patch size of the continuous model and investigate the quasistationary distribution of the number of individuals for patch sizes above the critical threshold. PMID:
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物理化学题目！！！求解答
某一级反应A---&产物，初始速率为1×10&#7旦龚测夹爻蝗诧伟超连10;-3mol·dmˆ-1·minˆ-1,1h后速率变为0.25×10ˆ-3mol·dmˆ-1·minˆ-1。求k
半衰期（t½）
初始浓度。要详细过程
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由一级反应可知，反应速率r=kc，设初始浓度为c0，1h后发现速率变为原来的1/4，那么此时的浓度为1/4c0，反应掉3/4co,对一级反应有公式ln（co/(co-x))=kt,（推导过程略），式中x为3/4c0，t=60min，求得k=0.0231minˆ-1，然后代入公式r=kc可求得co=0.0433mol·dmˆ旦龚测夹爻蝗诧伟超连-1。由ln（co/(co-x))=kt，令x=0.5co，代入即可求得半衰期t½=30min.
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单位应该是mol·dmˆ-3·minˆ-1ln(c0/c)=ktln(1×10ˆ-3/0.25×10ˆ-旦龚测夹爻蝗诧伟超连3)=k*60k=0.0231minˆ-1t1/2=ln2/k=ln2/0.0231=30min
一、一个实心小球先后放入盛有足够的水和足够多的酒精的两个容器中，小球受到的力分别是0.9牛和0.8牛，酒精的密谋为0.8×103 kg/m3。
1．分析小球在水中和在酒精中的浮沉状态
2．求小球的密度
解：假设小球在水中和在酒精中均不漂浮，或悬浮或一漂一悬，则应有：
因与题目已知条件矛盾，故不可能；
假设小球在水中和在酒精中均为沉底，则应有：
因与题目已知条件矛盾，故也不可能。
由以上分析可知：小球在水中和在酒精中时，只能是一漂一沉。
又因为 ，所以小球在水中一定是漂浮，在酒精中一定是沉底的。
(2)因小球在水中漂浮，
由已知条件：
将②式代入①式得：
二、体积为1.0×10-3m3的正方体木块，投入如图1所示装有水的容器中，静止后露出水面...
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出门在外也不愁All papers
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Coupled HBO and NBO variations in the Z source GX 5-1: inner accretion
disk as the location of QPOs
Abstract: The simultaneous and coupled evolution of horizontal branch oscillation (HBO)
and normal branch oscillation (NBO) in Z-type sources suggests that the
production of HBO is connected to NBO and is caused by changes in the
physical/radiative properties of the inner accretion disk, although there is a
lack of substantial spectral evidence to support this. In this {\it Letter}, we
present the results of an analysis of a RXTE observation of a Z source GX~5-1,
where the 6 Hz NBO is simultaneously detected along with a HBO at 51 Hz. The
variations in the intensity and the associated power density spectrum indicate
that the HBO and NBO are strongly coupled, originating from the same location
in the inner accretion disk. The absence of HBO and NBO in the lower energy
bands, an increase in the rms amplitude with energy and a smooth transition
among them suggest that they are produced in the hot inner regions of the
accretion disk. Based on a spectral analysis, we found a signature of changing
or physically modified inner disk front during the coupled HBO and NBO
evolution. We explore the various models to explain the observed phenomenon and
propose that the NBO is affiliated to the oscillations in the thick/puffed-up
inner region of the accretion disk.
High Energy Astrophysical Phenomena (astro-ph.HE)
[astro-ph.HE]
[astro-ph.HE] for this version)
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From: Kandulapati Sriram []
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